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| 1 | Suppression of m6A reader Ythdf2 promotes hematopoietic stem cell expansion显示文摘 | Zhenrui Li Pengxu Qian Wanqing Shao Hailing Shi Xi C. He Madelaine Gogol Zulin Yu Yongfu Wang Meijie Qi Yunfei Zhu John M. Perry Kai Zhang Fang Tao Kun Zhou Deqing Hu Yingli Han Chongbei Zhao Richard Alexander Hanzhang Xu Shiyuan Chen Allison Peak Kathyrn Hall Michael Peterson Anoja Perera Jeffrey S. Haug Tari Parmely Hua Li Bin Shen Julia Zeitlinger Chuan He Linheng Li | 2018 | Cell Research2018，28，9： | 18 |
| 2 | A kinetic study of the reaction of ozone with ethylene in a smog chamber under atmospheric conditions显示文摘Ozone is one of the key species in the processes of atmospheric chemistry, which can be taken as an indicator of oxidation capacity in the troposphere. The reaction of ozone with reactive gases is an important process in the troposphere. Experimental simulation equipment of smog chamber for atmospheric reactions is used to study the reaction of ozone with ethylene in real atmospheric environment with ozone concentrations of 100―200 ppb. The concentrations of ozone and ethylene were moni-tored during the reaction with the combination of Model 49C-O_3 Analyzer and GC-FID. A rate constant of 1.01×10^(-18) (cm^3·mol^(-1)·s-(~1)) was obtained at 286.5 K, under condition of which the half-life of ozone was 88 min. The results obtained from our experiments are in excellent agreement with those reported previously by other researchers under extremely low pressure in terms of matrixisolation technology. This demonstrates that our equipment of smog chamber for atmospheric reactions is reliable, which can be used for further research of the processes of atmospheric reactions. | XU Yongfu JIA Long GE Maofa DU Lin WANG Gengchen WANG Dianxun | 2006 | Chinese Science Bulletin2006，51，23： | 16 |
| 3 | Strategies to approach high performance in Cr^(3+)-doped phosphors for high-power NIR-LED light sources显示文摘Broadband near-infrared(NIR)-emitting phosphors are key for next-generation smart NIR light sources based on blue LEDs.To achieve excellent NIR phosphors,we propose a strategy of enhancing the crystallinity,modifying the micromorphology,and maintaining the valence state of Cr^(3+) in Ca_(3)Sc_(2)Si_(3)O_(12) garnet(CSSG).By adding fluxes and sintering in a reducing atmosphere,the internal quantum efficiency(IQE)is greatly enhanced to 92.3%.The optimized CSSG:6% Cr^(3+) exhibits excellent thermal stability.At 150℃,97.4% of the NIR emission at room temperature can be maintained.The fabricated NIR-LED device emits a high optical power of 109.9mW at 520 mA.The performances of both the achieved phosphor and the NIR-LED are almost the best results until now.The mechanism for the optimization is investigated.An application of the NIR-LED light source is demonstrated. | Zhenwei Jia Chenxu Yuan Yongfu Liu Xiao-Jun Wang Peng Sun Lei Wang Haochuan Jiang Jun Jiang | 2020 | Light(Science & Applications)2020，9，1： | 16 |
| 4 | Tomato SlAN11 regulates flavonoid biosynthesis and seed dormancy by interaction with bHLH proteins but not with MYB proteins显示文摘The flavonoid compounds are important secondary metabolites with versatile human nutritive benefits and fulfill a multitude of functions during plant growth and development.The abundance of different flavonoid compounds are finely tuned with species-specific pattern by a ternary MBW complex,which consists of a MYB,a bHLH,and a WD40 protein,but the essential role of SlAN11,which is a WD40 protein,is not fully understood in tomato until now.In this study,a tomato WD40 protein named as SlAN11 was characterized as an effective transcription regulator to promote plant anthocyanin and seed proanthocyanidin(PA)contents,with late flavonoid biosynthetic genes activated in 35S::SlAN11 transgenic lines,while the dihydroflavonol flow to the accumulation of flavonols or their glycosylated derivatives was reduced by repressing the expression of SlFLS in this SlAN11-overexpressed lines.The above changes were reversed in 35S::SlAN11-RNAi transgenic lines except remained levels of flavonol compounds and SlFLS expression.Interestingly,our data revealed that SlAN11 gene could affect seed dormancy by regulating the expressions of abscisic acid(ABA)signaling-related genes SlABI3 and SlABI5,and the sensitivity to ABA treatment in seed germination is conversely changed by SlAN11-overexpressed or-downregulated lines.Yeast two-hybrid assays demonstrated that SlAN11 interacted with bHLH but not with MYB proteins in the ternary MBW complex,whereas bHLH interacted with MYB in tomato.Our results indicated that low level of anthocyanins in tomato fruits,with low expression of bHLH(SlTT8)and MYB(SlANT1 and SlAN2)genes,remain unchanged upon modification of SlAN11 gene alone in the transgenic lines.These results suggest that the tomato WD40 protein SlAN11,coordinating with bHLH and MYB proteins,plays a crucial role in the fine adjustment of the flavonoid biosynthesis and seed dormancy in tomato. | Yongfeng Gao Jikai Liu Yongfu Chen Hai Tang Yang Wang Yongmei He Yongbin Ou Xiaochun Sun Songhu Wang Yinan Yao | 2018 | Horticulture Research2018，5，1： | 13 |
| 5 | Numerical study on ULF waves in a dipole field excited by sudden impulse显示文摘A three-dimensional numerical model is employed to investigate ULF waves ex-cited by the sudden impulse (SI) of the solar wind dynamic pressure interacting with a dipole magnetosphere. We focus on the solar wind-magnetosphere energy coupling through ULF waves, and the influences of the SI spectrum on the cavity mode structure and the energy deposition due to field line resonances (FLRs) in the magnetosphere. The numerical results show that for a given SI lasting for 1 min with amplitude of 50 mV/m impinging on the subsolar magnetopause, the total ULF energy transported from the solar wind to the magnetosphere is about the magni-tude of 1014 J. The efficiency of the solar wind energy input is around 1%, which depends little on the location of the magnetopause in the model. It is also found that the energy of the cavity mode is confined in the region near the magnetopause, whereas, the energy of the toroidal mode may be distributed among a few specific L-shells. With a given size of the model magnetosphere and plasma density distri-bution, it is shown that the fundamental eigenfrequency of the cavity mode and the central locations of the FLRs do not vary noticeably with the power spectrum of the SI. It is worth noting that the spectrum of the SI affects the excitation of higher harmonics of the global cavity mode. The broader the bandwidth of the SI is, the higher harmonics of cavity mode could be excited. Meanwhile, the corresponding FLRs regions are broadened at the same time, which implies that the global cavity modes and toroidal modes can resonate on more magnetic L-shells when more harmonics of the global cavity modes appear. | YANG Biao FU SuiYan ZONG QiuGang WANG YongFu ZHOU XuZhi PU ZuYin XIE Lun | 2008 | Science China(Technological Sciences)2008，51，10： | 12 |
| 6 | Fast acceleration of “killer” electrons and energetic ions by interplanetary shock stimulated ULF waves in the inner magnetosphere显示文摘Energetic electrons and ions in the Van Allen radiation belt are the number one space weather threat. Understanding how these energetic particles are accelerated within the Van Allen radiation belt is one of the major challenges in space physics. This paper reviews the recent progress on the fast acceleration of 'killer' electrons and energetic ions by ultralow frequency (ULF) waves stimulated by the interplanetary shock in the inner magnetosphere. Very low frequency (VLF) wave-particle interaction is considered to be one of the primary electron acceleration mechanisms because electron cyclotron resonances can easily occur in the VLF frequency range. Recently, using four Cluster spacecraft observations, we have found that, after interplanetary shocks impact the Earth’s magnetosphere, energetic electrons in the radiation belt are accelerated almost immediately and continue to accelerate for a few hours. The time scale (a few days) for traditional acceleration mechanisms, based on VLF wave-particle interactions to accelerate electrons to relativistic energies, is too long to explain our observations. Furthermore, we have found that interplanetary shocks or solar wind pressure pulses, with even small dynamic pressure changes, can play a non-negligible role in radiation belt dynamics. Interplanetary shocks interaction with the Earth’s magnetosphere manifests many fundamental space physics phenomena including energetic particle acceleration. The mechanism of fast acceleration of energetic electrons in the radiation belt responding to interplanetary shock impacts consists of three contributing parts: (1) the initial adiabatic acceleration due to strong shock-related magnetic field compression; (2) followed by the drift-resonant acceleration with poloidal ULF waves excited at different L-shells; and (3) particle acceleration due to the quickly damping electric fields associated with ULF waves. Particles end up with a net acceleration because they gain more energy in the first half of this cycle than they lose in the second. The results reported in this paper cast a new light on understanding the acceleration of energetic particles in the Earth’s Van Allen radiation belt. The results of this study can likewise be applied to interplanetary shock interaction with other planets such as Mercury, Jupiter, Saturn, Uranus and Neptune, and other astrophysical objects with magnetic fields. | ZONG QiuGang WANG YongFu YUAN ChongJing YANG Biao WANG ChenRui ZHANG XiangYun | 2011 | Chinese Science Bulletin2011，56，12： | 11 |
| 7 | Multi-spacecraft observations of ULF waves during the recovery phase of magnetic storm on October 30, 2003显示文摘Based on observations obtained by Cluster C1, GOES 10, 12, and Polar, the global ULF wave properties are studied during the recovery phase of a very intense magnetic storm-Halloween storm (October 31, 2003, 21:00-23:00 UT). The results indicate that the ULF waves’ properties observed by different satellites, such as amplitude, period, etc. show large variations. This can be interpreted as that Field Line Resonance (FLR) might take place in the region where Cluster C1 passed. The compressional wave of the cavity mode coupled with FLR’s shear Alfven wave and fed energy to the latter, forming a large-amplitude toroidal mode. From the point of period, Cluster C1 observed the shortest period, GOES 10, 12 observed the middle, while Polar observed the longest. The wave period of toroidal mode observed by Cluster C1 kept almost unchanging when Cluster C1 passed L range from 11.7 to 5.3. Using the Squared Wavelet Coherence analysis method, we estimated that the FLR region in the dayside magnetosphere could expand to at least 4 local time widths. The toroidal mode observed by Polar was a standing wave, while the pol-oidal mode was a propagating wave, the observation results could be well ex-plained by the waveguide mode theory. Since the solarwind speed Vx was -800 km/s and the dynamic pressure varied little, we speculated that the source of the ULF wave was the Kelvin-Helmholtz instability at the magnetopause triggered by high speed solarwind. | YongFu Wang SuiYan Fu QiuGang Zong Biao Yang ZuYin Pu Lun Xie XuZhi Zhou | 2008 | Science China(Technological Sciences)2008，51，10： | 11 |
| 8 | Influence of solar wind dynamic pressure on geomagnetic Dst index during various magnetic storms显示文摘The Dst index,designed as a proxy of ring current intensity,is known to be also affected by other magnetospheric current systems,e.g.magnetopause current.The pressure-corrected Dst index is obtained by removing the effects of the solar wind dynamic pressure and the quiet time ring current.However,all previous studies treated the correction coefficient as an averaged parameter for storms of different intensity.In this paper,based on the Burton's equations and employing two independent methods,we will show a positive correlation between pressure-correction coefficient b and the intensity of the storms.We divided our storm database(872 storms in total) into three categories according to the intensity of storms.In order to improve the accuracy of calculating,we also used the higher-resolution SYM-H index data instead of Dst index to compute the corrected Dst index during different storms.Furthermore,we are able to provide corrected magnetic storm index with high-time resolution(-1 min). | ZHAO Hong ZONG QiuGang WEI Yong WANG YongFu | 2011 | Science China(Technological Sciences)2011，54，6： | 10 |
| 9 | Radial propagation of magnetospheric substorm-injected energetic electrons observed using a BD-IES instrument and Van Allen Probes显示文摘In cases where substorm injections can be observed simultaneously by multiple spacecraft,they can help elucidate the potential mechanisms of particle transport and energization,of great importance to understanding and modeling the magnetosphere.In this paper,using data returned from the BeiDa-IES(BD-IES) instrument onboard a satellite in an inclined(55°) geosynchronous orbit(IGSO),in combination with two geo-transfer orbiting(GTO) satellite Van Allen Probes(A and B),we analyze a substorm injection event that occurred on the 16 th of October 2015.During this substorm injection,the IGSO onboard BD-IES was outbound,while both Van Allen Probe satellites(A and B) were inbound,a configuration of multiple trajectories that provides a unique opportunity to simultaneously investigate both the inward and outward radial propagation of substorm injection.Indicated by AE/AL indices,this substorm was closely related to an IMF/solar wind discontinuity that showed a sharp change in IMF Bz direction to the north.The innermost signature of this substorm injection was detected by Van Allen Probes A and B at L-3.7,while the outermost signature was observed by the onboard BD-IES instrument at L~\0.These data indicate that the substorm had a global,rather than just local,effect.Finally,we suggest that electric fields carried by fast-mode compressional waves around the substorm injection are the most likely candidate mechanism for the electron injection signatures observed in the inner- and outermost inner magnetosphere. | ZONG QiuGang HAO YiXin ZOU Hong FU SuiYan ZHOU XuZhi REN Jie WANG LingHua YUAN ChongJing LIU ZhiYang JIA XiangHong QUAN Lin LIU Ying WANG YongFu | 2016 | Science China Earth Sciences2016，59，7： | 8 |
| 10 | Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock显示文摘Interplanetary shock can greatly disturb the Earth's magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03―45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8―16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 cm-3, compared to the typical number density of 0.7 cm-3. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 cm-3. The inferred ionospheric O+ density after the interplanetary shock impact reaches the maximum value of 1.2 cm-3 on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton's temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8―16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8―16 LT) with a value of 2 kHz. | YUE Chao ZONG QiuGangt WANG YongFu | 2009 | Chinese Science Bulletin2009，54，22： | 7 |
| 11 | Ultra low frequency waves impact on radiation belt energetic particles显示文摘One of the most fundamental important issues in the space physics is to understand how solar wind energy transports into the inner magnetosphere.Ultra low frequency(ULF)wave in the magnetosphere and its impact on energetic particles,such as the wave-particle resonance,modulation,and particle acceleration,are extremely important topics in the Earth’s radiation belt dynamics and solar wind― magnetospheric coupling.In this review,we briefly introduce the recent advances on ULF waves study. Further,we will explore the density structures and ion compositions around the plasmaspheric boundary layer(PBL)and discuss its possible relation to the ULF waves. | ZONG QiuGang HAO YongQiang WANG YongFu | 2009 | Science China(Technological Sciences)2009，52，12： | 7 |
| 12 | Ultra low frequency waves observed by Double Star TC-1 in the plasmasphere boundary layer显示文摘The characteristic and properties of ULF waves in the plasmasphere boundary layer during two very quiet periods are present. The ULF waves were detected by Double Star TC-1 when the spacecraft passed through the plasmasphere in an outbound and inbound trajectories, respectively. A clear association between the ULF waves and periodic variations of energetic ions fluxes was observed. The ob-servations showed that the wave frequency was higher inside the plasmasphere than outside. The mechanism generating these ULF waves and possible diagnos-ing of the 'classical plasmapause' location with the ULF wave were discussed. | XIE Lun ZHANG XiaoJia PU ZuYin WANG YongFu FU SuiYan ZONG QiuGang | 2008 | Science China(Technological Sciences)2008，51，10： | 7 |
| 13 | Application of seismic facies and attributes analysis on the identification of Permian igneous rock显示文摘Seismic facies and attributes analysis techniques are introduced.The geological characteristics of some oil fields in western China are used in conjunction with drilling results and logging data to identify the lithology,intrusion periods,and distribution range of the Permian igneous rocks in this area.The lithologic classification,the vertical and horizontal distribution,and the intrusion periods of igneous rock were deduced through this study.Combining seismic facies and attributes analysis based on optimization can describe the igneous rock in detail.This is an efficient way to identify lithology and intrusion periods.Using geological data and GR-DT logging cross-plots the Permian igneous rock from TP to TT was divided into three periods.The lithology of the first period is tuff and clasolite with a thickness ranging from 18 to 80 ms.The second is basalt with a thickness ranging from 0 to 20 ms.The third is tuff and clasolite and dacite whose thickness ranges from 60 to 80 ms.These results can help understand the clasolite trap with low amplitude and the lithologic trap of the Carboniferous and Silurian.They can also guide further oil and/or gas exploration. | Xu Yongzhong Yang Haijun Liu Yongfu Wang Shuangshuangx Wang Shuangshuang Yang Peng Zhao Jixiang | 2012 | International Journal of Mining Science and Technology2012，22，4： | 6 |
| 14 | Numerical simulation of magnetospheric ULF waves excited by positive and negative impulses of solar wind dynamic pressure显示文摘The sources of ultra low frequency (ULF) waves in the magnetosphere are generally believed to be either the external solar wind perturbations or the internal plasma instabilities. When a sudden impulse of the solar wind dynamic pressure impinges on the magnetopause, ULF waves might be excited and thus the solar wind energy is transported into the earth's magnetosphere. In this paper, we study the ULF waves excited by different kinds of sudden solar wind pressure impulses through an MHD simulation. We primarily focus on the responses of the earth's magnetosphere to positive/negative impulses of solar wind dynamic pressure, and positive-negative impulse pairs. The simulation results show that the ULF waves excited by positive and negative impulse have the same amplitude and frequency, with 180° difference in phase, if the amplitude and durations of the input impulses are the same. In addition, it is found that field line resonances (FLRs) occur at certain L-shell regions of the earth's magneto-sphere after the impact of different positive-negative impulse pairs, which appear to be related to the duration of the impulses and the time interval between the sequential impulses. Another result is that the energy from the solar wind could be transported deeper into the inner magnetosphere by an impulse pair than by a single pulse impact. The results presented in this paper could help us to better understand how energy is transported from solar wind to the earth's magnetosphere via ULF waves. Also, these results provide some new clues to understanding of how energetic particles in the inner magnetosphere response to different kinds of solar wind pressure impulse impacts including inter-planetary shocks. | ZHANG XiangYun ZONG QiuGang YANG Biao WANG YongFu | 2009 | Science China(Technological Sciences)2009，52，10： | 6 |
| 15 | Molecular properties, functions, and potential applications of NAD kinases显示文摘NAD kinase 催化 NAD (H) 的 phosphorylation 形成 NADP (H) ,用象 phosphoryl 施主的 ATP。导致 de novo NADP+/NADPH 生合成是唯一的关键酶的。象 NAD (H) 和 NADP (H) 那样的辅酶以他们的重要功能著名。最近的研究部分证明了 NAD kinase 在 NAD (H)/NADP (H) 变换的规定起一个关键作用。这里, NAD kinase 的分子的性质,生理的功能,和潜在的应用被讨论。 | Feng Shi Yongfu Li Ye Li Xiaoyuan Wang | 2009 | Acta Biochimica et Biophysica Sinica2009，41，5： | 6 |
| 16 | Supercapacitors based on high-surface-area graphene显示文摘Exfoliated graphite oxide was prepared by an improved Hummers method and was then reduced to graphene with hydrazine in the presence of ammonium hydroxide.N2adsorption–desorption measurement showed that graphene so obtained had a specific surface area as high as 818 m2/g.Galvanostatic charge/discharge curves demonstrated that the as-prepared graphene exhibited a specific capacitance of 186.9 F/g at a current density of 0.1 A/g and that about 96%of the specific capacitance was retained after 2000 cycles at a current density of 5 A/g. | ZHOU XiaoLin WANG Min LIAN Jie LIAN YongFu | 2014 | Science China(Technological Sciences)2014，57，2： | 6 |
| 17 | Dynamic variation and the fast acceleration of particles in Earth's radiation belt显示文摘We have quantitatively investigated the radiation belt's dynamic variations of 1.5-6.0 MeV electrons during 54 CME (coronal mass ejection)-driven storms from 1993 to 2003 and 26 CIR (corotating interaction region)-driven recurrent storms in 1995 by utilizing case and statistical studies based on the data from the SAMPEX satellite. It is found that the boundaries determined by fitting an exponential to the flux as a function of L shell obtained in this study agree with the observed outer and inner boundaries of the outer radiation belt. Furthermore, we have constructed the Radiation Belt Content (RBC) index by integrating the number density of electrons between those inner and outer boundaries. According to the ratio of the maximum RBC index during the recovery phase to the pre-storm average RBC index, we conclude that CME-driven storms produce more relativistic electrons than CIR-driven storms in the entire outer radiation belt, although the relativistic electron fluxes during CIR-related storms are much higher than those during CME-related storms at geosynchronous orbit. The physical radiation belt model STEERB is based on the three-dimensional Fokker-Planck equation and includes the physical processes of local wave-particle interactions, radial diffusion, and adiabatic transport. Due to the limitation of numerical schemes, formal radiation belt models do not include the cross diffusion term of local wave-particle interactions. The numerical experiments of STEERB have shown that the energetic electron fluxes can be overestimated by a factor of 5 or even several orders (depending on the pitch angle) if the cross diffusion term is ignored. This implies that the cross diffusion term is indispensable for the evaluation of radiation belt electron fluxes. Formal radiation belt models often adopt dipole magnetic field; the time varying Hilmer-Voigt geomagnetic field was adopted by the STEERB model, which self-consistently included the adiabatic transport process. The test simulations clearly indicate that the adiabatic process can significantly affect the evolution of radiation belt electrons. The interactions between interplanetary shocks and magnetosphere can excite ULF waves in the inner magnetosphere; the excited polodial mode ULF wave can cause the fast acceleration of 'killer electrons'. The acceleration mechanism of energetic electrons by poloidal and toroidal mode ULF wave is different at different L shells. The acceleration of energetic electrons by the toroidal mode ULF waves becomes important in the region with a larger L shell (the outer magnetosphere); in smaller L shell regions (the inner magnetosphere), the poloidal mode ULF becomes responsible for the acceleration of energetic electrons. | ZONG QiuGang YUAN ChongJing WANG YongFu SU ZhenPeng | 2013 | Science China Earth Sciences2013，56，7： | 5 |
| 18 | Study of the nose event on 11 April 2002 with UBK method显示文摘Nose event,which names after the nose-like shape of structures in ion spectrograms observed by satellite in the inner magnetosphere,refers to the deep inward penetration of ions from magnetotail at discrete energy bands.Nose events have been studied extensively both with observations and simulations since first discovered in 1970s.In this study we use the UBK method to model the different L-shell penetration characteristics for a multi-band nose event observed by Cluster/CODIF on April 11,2002.The modeled open-closed orbit separatrices are generally smaller than the observed L-shell penetrations for outbound crossing;the difference varies from 2.02 to 0.62 R E for different energy channels of H + bands and from 1.88 to 1.10 R E for O + band.The average difference is 1.46 R E.The separatrices for the inbound crossing are generally larger than those of outbound crossing and are more consistent with the observed L-shell penetration depths.The modeled open-closed orbit separatrices are smaller than the observed L-shell penetrations for 6.5-17.1 keV energy channels of H + bands but larger for 4.0-5.1 keV(due to closed banana orbits region) and 21.7-35.2 keV(due to energy increasing) energy channels of H + bands.For O + band,the difference between the modeled open-closed orbit separatrix and observed L-shell penetrations of 4.6 keV energy channel is larger(due to closed banana orbits region),the difference of 7.4 keV energy channel is smaller.The overall average difference is 0.043 R E for nose structures of inbound crossing.The discrepancies between the model and observation may come from the magnetic field and electric potential models we used.The formation of multi nose event and relations to the observed plasma flow vortices are discussed,the local intense E Y may relate to the formation of the observed multi nose structures. | WANG YongFu ZONG QiuGang | 2012 | Science China(Technological Sciences)2012，55，7： | 5 |
| 19 | High performance heterogeneous embedded computing: a review显示文摘As increasingly widening gap of computing demand and performance in embedded computing domain,heterogeneous computing architecture which delivers better performance as well as lower power in limited size is gaining more and more attention. At first,the heterogeneous computing model is presented. And the different tightly coupled single chip heterogeneous architectures and their application domain are introduced. Then,task partitioning methods are described. Several programming model technology are analyzed and discussed. Finally,main challenges and future perspective of High Performance Embedded Computing(HPEC) are summarized. | HE Yongfu WANG Shaojun PENG Yu | 2014 | Instrumentation2014，1，2： | 5 |
| 20 | Statistical study of the properties of the magnetic field and plasma in the earth's magnetotail near lunar orbit显示文摘基于数据获得了由的磁场和血浆在月亮的轨道附近的 magnetotail 的在 19921995 的 GEOTAIL 和风 in19942009,磁场和血浆性质用迭加的时代分析统计上被学习。结果近显示出那 0 ?? 邬吗?? | TIAN Tian ZONG QiuGang WANG YongFu FEI ZengPing | 2012 | Science China(Technological Sciences)2012，55，9： | 5 |
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